UPDATE on NEW PHYSICS AT COLLIDERS ANTONIO MASIERO UNIV. OF PADUA and INFN, PADUA LCWS 07, DESY May 30, 2007
UPDATE on NEW PHYSICS AT COLLIDERS
ANTONIO MASIEROUNIV. OF PADUA
andINFN, PADUA
LCWS 07, DESY May 30, 2007
WHY TO GO BEYOND THE SM
“OBSERVATIONAL” REASONS
•HIGH ENERGY PHYSICS
(but AFB……)
•FCNC, CPNO (but b sqq penguin,Vub …)
•HIGH PRECISION LOW-EN.
NO (but (g-2) …)
•NEUTRINO PHYSICS YE m 0, 0
•COSMO - PARTICLE PHYSICS
YE (DM, ∆B cosm, INFLAT., DE)
Z bbNO
NO
NO
YES
YES
THEORETICAL REASONS•INTRINSIC INCONSISTENCY OF SM AS QFT
(spont. broken gauge theory without anomalies)
•NO ANSWER TO QUESTIONS THAT “WE” CONSIDER “FUNDAMENTAL” QUESTIONS TO BE ANSWERED BY A “FUNDAMENTAL” THEORY
(hierarchy, unification, flavor)
NO
YES
FROM DETERMINATION TO VERIFICATION OF THE CKM PATTERN FOR HADRONIC
FLAVOR DESCRIPTION
TREE LEVEL
ONE - LOOP
A. BURAS et al.
Single channels
understood?
Allowed to take the avg.?
FLAVOR BLINDNESS OF THE NP AT THE ELW. SCALE?
• THREE DECADES OF FLAVOR TESTS ( Redundant determination of the UT triangle verification of the SM, theoretically and experimentally “high precision” FCNC tests, ex. b s + γ, CP violating flavor conserving and flavor changing tests, lepton flavor violating (LFV) processes, …) clearly state that:
• A) in the HADRONIC SECTOR the CKM flavor pattern of the SM represents the main bulk of the flavor structure and of CP violation;
• B) in the LEPTONIC SECTOR: although neutrino flavors exhibit large admixtures, LFV, i.e. non – conservation of individual lepton flavor numbers in FCNC transitions among charged leptons, is extremely small: once again the SM is right ( to first approximation) predicting negligibly small LFV
What to make of this triumph of the CKM pattern in flavor tests?
New Physics at the Elw. Scale is Flavor Blind CKM exhausts the flavor changing pattern at the elw. Scale
MINIMAL FLAVOR VIOLATION
New Physics introduces
NEW FLAVOR SOURCES in addition to the CKM pattern. They give rise to contributions which are <10 -20% in the “flavor observables” which have already been observed!
MFV : Flavor originates only from the SM Yukawa coupl.
What a SuperB can do in testing CMFVL. Silvestrini at SuperB IV
SuperB vs. LHC Sensitivity Reach in testing SUSY
SuperB can probe MFV ( with small-moderate tan) for TeV squarks; for a generic non-MFV MSSM sensitivity to squark masses > 100 TeV ! L. Silvestrini
THE FATE OF LEPTON NUMBERL VIOLATED L CONSERVED
Majorana ferm. Dirac ferm.(dull option)
SMALLNESS of m h LH R m=h H M5 eV h10-11
EXTRA-DIM. R in the bulk: small overlap?PRESENCE OF A NEW PHYSICAL MASS SCALE
NEW HIGH SCALE
SEE - SAW MECHAN.Minkowski; Gell-Mann, Ramond, SlansKy, Vanagida
ENLARGEMENT OF THE FERMIONIC SPECTRUM
MR R + h L R
L ~O h
R h M
RL
NEW LOW SCALE
MAJORON MODELS
Gelmini, Roncadelli
ENLARGEMENT OF THE HIGGS SCALAR SECTOR
h L L m= h
N.B.: EXCLUDED BY LEP!
R
LRModels?
µ e+ in SUSYGUT: past and future
CFMVCALIBBI, FACCIA, A.M., VEMPATI
SUSY SEESAW AND LARGE LFV ENHANCEMENT
LFV from SUSY GUTs Lorenzo Calibbi
and PRISM/PRIME conversion experiment
LFV from SUSY GUTs Lorenzo Calibbi
and the Super B (and Flavour) factories
H mediated LFV SUSY contributions to RK
Extension to B l deviation from universality Isidori, Paradisi
PARADISI, A.M.,PETRONZIO
A FUTURE FOR FLAVOR PHYSICS IN OUR SEARCH BEYOND THE SM?
• The traditional competition between direct and indirect (FCNC, CPV) searches to establish who is going to see the new physics first is no longer the priority, rather
• COMPLEMENTARITY between direct and indirect searches for New Physics is the key-word
• Twofold meaning of such complementarity:
i) synergy in “reconstructing” the “fundamental theory” staying behind the signatures of NP;
ii) coverage of complementary areas of the NP parameter space ( ex.: multi-TeV SUSY physics)
MICRO MACROPARTICLE PHYSICS COSMOLOGY
GWS STANDARD MODEL HOT BIG BANG STANDARD MODEL
HAPPY MARRIAGE Ex: NUCLEOSYNTHESIS
BUT ALSO POINTS OF FRICTION
-COSMIC MATTER-ANTIMATTER ASYMMETRY
-INFLATION
- DARK MATTER + DARK ENERGY
“OBSERVATIONAL” EVIDENCE FOR NEW PHYSICS BEYOND
THE (PARTICLE PHYSICS) STANDARD MODEL
The energy budget of the Universe
DM: the most impressive evidence at the “quantitative” and “qualitative” levels of
New Physics beyond SM
• QUANTITATIVE: Taking into account the latest WMAP data which in combination with LSS data provide stringent bounds on DM and B EVIDENCE FOR NON-BARYONIC DM AT MORE THAN 10 STANDARD DEVIATIONS!! THE SM DOES NOT PROVIDE ANY CANDIDATE FOR SUCH NON-BARYONIC DM
• QUALITATIVE: it is NOT enough to provide a mass to neutrinos to obtain a valid DM candidate; LSS formation requires DM to be COLD NEW PARTICLES NOT INCLUDED IN THE SPECTRUM OF THE FUNDAMENTAL BUILDING BLOCKS OF THE SM !
STABLE ELW. SCALE WIMPs from PARTICLE PHYSICS
1) ENLARGEMENT OF THE SM
SUSY EXTRA DIM. LITTLE HIGGS. (x, ) (x, ji) SM part + new part
Anticomm. New bosonic to cancel 2
Coord. Coord. at 1-Loop2) SELECTION RULE
DISCRETE SYMM.
STABLE NEW PART.
R-PARITY LSP KK-PARITY LKP T-PARITY LTP
Neutralino spin 1/2 spin1 spin0
3) FIND REGION (S) PARAM. SPACE WHERE THE “L” NEW PART. IS NEUTRAL + ΩL h2 OK
* But abandoning gaugino-masss unif. Possible to have mLSP down to 7 GeV
mLSP
~100 - 200
GeV *
mLKP
~600 - 800
GeV
mLTP
~400 - 800
GeV
Bottino, Donato, Fornengo, Scopel
SEARCHING FOR WIMPs
WIMPS HYPOTHESIS
DM made of particles with mass 10Gev - 1Tev
ELW scale
With WEAK INTERACT.
LHC, ILC may PRODUCE WIMPS
WIMPS escape the detector MISSING ENERGY
SIGNATURE
FROM “KNOWN” COSM. ABUNDANCE OF WIMPs PREDICTION FOR WIMP PRODUCTION AT COLLIDERS WITHOUT SPECYFING THE PART. PHYSICS MODEL OF WIMPs
BIRKEDAL, MATCHEV, PERELSTEIN , FENG,SU, TAKAYAMA
Carena
CARENA, HOOPER, VALLINOTTO 06
CARENA at MORIOND 07
Carlos Wagner
CARENA, BALAZS, WAGNER
A.M., PROFUMO, ULLIO
A.M., PROFUMO,ULLIO
THE “WHY NOW” PROBLEM
DM DEDO THEY “KNOW” EACH OTHER?
DIRECT INTERACTION (quintessence) WITH DARK MATTER DANGER:
Very LIGHTm ~ H0
-1 ~ 10-33 eVThreat of violation of the equivalence principle, constancy of the fundamental “constants”, …CARROLL
INFLUENCE OF ON THE NATURE AND THE ABUNDANCE OF CDM
Modifications of the standard picture of WIMPs FREEZE - OUT
CDM CANDIDATES
CATENA, FORNENGO, A.M., PIETRONI, ROSATI, SCHELKE
The Energy Scale from the“Observational” New Physics
neutrino masses
dark matter
baryogenesis
inflation
NO NEED FOR THE NP SCALE TO BE CLOSE TO THE ELW. SCALE
The Energy Scale from the “Theoretical” New Physics
Stabilization of the electroweak symmetry breaking at MW calls for an ULTRAVIOLET COMPLETION of the SM already
at the TeV scale +
CORRECT GRAND UNIFICATION “CALLS” FOR NEW PARTICLES AT THE ELW. SCALE (?)
UV COMPLETION OF THE SM AND THE ORIGIN OF THE ELW. SYMMETRY BREAKING
DYNAMICS RESPONSIBLE FOR
ELW. SYMMETRY BREAKING
WEAKLY COUPLED STRONGLY COUPLED
LIGHT HIGGS
Favored by LEP1
NEW QCD SCALED AT 1 TEV
Disfavored by LEP1
THE LOW-ENERGY SUSY TENSIONbetween the UV COMPLETION SCALE and the
POST-LEP SUSY EXCLUSIONS
Giudice, Rattazzi Zwirner
ELW. SYMM. BREAKING STABILIZATION VS. FLAVOR PROTECTION: THE SCALE TENSION
UV SM COMPLETION TO STABILIZE THE ELW. SYMM. BREAKING: UV ~ O(1 TeV)
Isidori
SUSY
Hitoshi Murayama
WHICH SUSYHIDDEN
SECTOR SUSY BREAKING AT
SCALE F
OBSERVABLE SECTOR
SM + superpartnersMSSM : minimal content
of superfields
ME
SS
EN
GE
RSF = MW MPl
GRAVITY
Mgravitino ~ F/MPl ~ (102 -103) GeV
GAUGE INTERACTIONS
F = (105 - 106) GeV
Mgravitino ~ F/MPl ~
(102 - 103)eV
Carena
Giudice, Grojean, ALEX POMAROL,Rattazzi
GGPR
Toni Gheghetta
at Moriond 07
GABELLA, GHERGHETTA, GIEDT
Gabella et al.
FCNC, CP ≠, (g-2), ()0 m n …
LINKED TO COSMOLOGICAL EVOLUTION
Possible interplay with dynamical DE
NEWPHYSICS AT
THE ELW SCALE
DM - FLAVOR
for DISCOVERY
and/or FUND. TH.
RECONSTRUCTION
A MAJOR LEAP AHEAD IS NEEDED
LFV
BARYO- LEPTO- GENESIS
TEVATRON ILC